Stellar-Mass, Intermediate-Mass, and Supermassive Black Holes ー Overview ー
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Transcript of Stellar-Mass, Intermediate-Mass, and Supermassive Black Holes ー Overview ー
Stellar-Mass, Intermediate-Mass,Stellar-Mass, Intermediate-Mass,
and Supermassive Black Holesand Supermassive Black Holes
ー ー Overview Overview ーー Shin Mineshige (Yukawa Institute, Kyoto)
• Comparative study of astrophysical BHs • Beyond the standard disk model• BH formation & evolution
Black Hole Candidates
BHs can be found in many places and seem to have had great influence on the evolution of the universe.
mass (solar m
ass)
Our Galaxy nearby galaxies distant galaxies early universe100
102
104
106
108
stellar-mass BHs
intermediate-mass BHs (ULXs)
galactic nuclei
gamma-ray bursts (?)
before 〜 1995 after〜 1995
(NLS1s)
(unknown populations??)
(c) K. Makishima
(quasars)
Sgr A*
Comparative study of Comparative study of astrophysical black holesastrophysical black holes
If physics is common, then we expect
Soft (blackbody) comp. ⇒ Teff ∝ MBH-1/4
Hard (power-law) comp. ⇒ T ∝ MBH0
Accretion-rate dependent evolution also in ULXs & AGNs
Soft-state AGNs?
Variability timescale ∝ MBH
X-ray nova (XN)-type eruptions in AGN?
Common physics? Fundamental differences?
Accretion rate-dependent Accretion rate-dependent evolution in X-ray binariesevolution in X-ray binaries
Similar transition in other BH objects?
Very high state
High/soft state
Intermediate state
Low/hard state
Quiescence
Esin et al. (1997)
Slim disk (+corona)
Standard disk+corona
Standard disk
ADAF/CDAF/MHD Flow
?m .
Session 1 (10/28 morning)
Soft-state AGN?Soft-state AGN?
We expect the presence of soft-state AGNs!!
(1) Standard disk solution exists for AGN parameters.
(2) Disk-corona model also predicts soft-state AGN.
Liu et al. (ApJ 572, L173, 2002; ApJ 587, 571, 2003)
Simple disk-corona model based on the analogy with solar corona Reconnection heating = Compton cooling in corona Conduction heating = evaporation cooling in chromosphere
(3) (Some of) narrow-line Sy 1s show soft-state spectra.
Session 7 (10/31 morning)
Variability timescaleVariability timescale ∝∝ MMBHBH ?? Hayashida et al. (1998)
×104
×106
Compare Fourier frequency at a fixed normalized PSD.
Variability t.s. ∝(r3/GMBH)1/2 ∝MB
H (r/rs)3/2
Such a scaling law is expected, if physics underlying variability is the same.
Session 5 (10/30, morning)
X-ray nova type eruptions in X-ray nova type eruptions in AGN?AGN? Mineshige & Shields (ApJ 1990)
Limit-cycle instability
Cool disks (below 104 K) are unstable, giving rise to quasi-periodic outbursts.
⇒ Dwarf-nova & X-ray nova eruptions
AGN disks are also unstable at ~ 0.1 pc.
⇒ Possible AGN eruptions, but no such report so far. Just missing? Or instability is somehow suppressed?
Σ
M・
4/34/1
2Edd
2/1
sun8
BHeff pc 1.0 /1010
(K) 2500~
r
cL
M
M
MT
Osaki (74), Hoshi (79), Meyer & Meyer-Hofmeister (81)
Beyond the standard modelBeyond the standard model
The standard disk model is very successful buThe standard disk model is very successful bu
t is not an only solution.t is not an only solution.
What differs in other disk models?What differs in other disk models?
Slim disk (near-critical accretion flow)Slim disk (near-critical accretion flow) Radiatively inefficient flow Radiatively inefficient flow (ADAF/CDAF/MHD flow (ADAF/CDAF/MHD flow …)…) Neutrino-cooled accretion flowNeutrino-cooled accretion flow
Various disk modelsVarious disk models
Kato, Fukue & Mineshige (1998), Narayan, Piran & Kumar
(2001)
standard disk : Qvis = Qrad ≫ Qadv , Qν
ADAF (CDAF): Qvis = Qadv(sgas) ≫ Q rad , Qν
slim disk : Qvis = Qadv(srad) ≫Q rad , Qν
NDAF : Qvis = Qν ≫ Qadv , Q rad
Radiation
Fluid
Trapped photons
Grav. energy
→
→
→
Neutrinos
→
Qadv ~ ΣTvr (ds/dr ) = advection term
Qvis = viscous heating
Qrad ( Qν ) = radiative (neutrino) cooling
How can we distinguish standard and How can we distinguish standard and slim disks?slim disks? Manmoto & Mineshige (in prep.)
Temp. profiles
Teff ∝ r -3/4 (low M)
Teff ∝ r -1/2 (high M)
Disk inner edge
rin ~ 3rS (low M)
rin ~ rS (high M)
3 rS
. M/(LE/c2)=1,10,102,103
MBH=105Msun
.
.
.
.
Disk inner edge shifts from 3rS to ~ rS as L increases.
BHCs inBHCs in TTinin- - LL diagram diagram (Watarai, Mizuno, Mineshige, ApJ 549, L77, 200
1)
r in=co
nst
rin decreases
as L increases
Sessions 1 & 2 (10/28)
Spectral states at Spectral states at LL ~~ LLEddEdd
Slim-disk state Blackbody-like spectra Small variability
Very high state Three spectral components:
BB + power-law + Compton. BB Large variability
High/soft state
Low/hard state
….
Apparently looks like the low-hard state.
Apparently looks like the high-soft state.
Kubota et al. (2002)
M .
Sessions 1 & 2 (10/28)
Radiatively inefficient flow Radiatively inefficient flow (ADAF, CDA(ADAF, CDAF, …)F, …)
Advection-Dominated Accretion Flow (ADAF) Low emissivity high temp. geometrically thick flow
Convection (CDAF)
Outflow (ADIOS)
Magnetized (MHD) flow Low emissivity large pgas large pmag enhanced mag. activity
Ichimaru (1977); Abramowicz et al.
(1995); Narayan & Yi (1994, 1995)
1D (radial) model
3D simulation
Sessions 4 (10/29)
Simulation movie: magnetic-tower
jetKato, Mineshige & Shibata (2003)
Sessions 3 & 4 (10/29)
Formation/evolution of BHsFormation/evolution of BHs
Formation
SN explosion can generate a stellar-mass BH.
More massive BHs can be created either by a collapse
of supermassive star or merger of lower-mass object
s.
Evolution Cosmological growth of BHs and AGN phenominon. Co-evolution of galaxies and BHs.
Were supermassive BHs generated from IMBHs?
Merger scenarios for forming SuperMerger scenarios for forming Supermassive BHsmassive BHs (cf. Ebisuzaki et al. 2000)
Status at the End of Starburst Star Clusters with IMBH Sink of Star Clusters with IMBHs
into Galaxy CenterMerge of Star Clusters and
Sink of IMBHs into Galaxy Center
Merge of IMBHs into a Super Massive BH by Radiation of Gravitational Wave
67
8
9
GlobularCluster
BulgeSuper MassiveBlack Hole
Jet, Radiation
Formation of Bulge, Globular Clusters and AGN
10 QSO in Early Universe
coutersy of T. Tsuru
Sessions 6 (10/30, afternoon)
Cosmological evolution of Cosmological evolution of AGN spatial densityAGN spatial density
Number density of higher luminosity AGNs peaked at higher redshifts.
Ueda et al. (2003)
Similar evolutions are found for star-formation rates.
Sessions 6 (10/30, afternoon)
Summary:Summary: Outstanding Outstanding issuesissues
Discoveries of intermediate-mass black hole candidates prompt thorough
comparative study of different BHs.
Interesting subclass: narrow-line Seyfert 1s (NLS1s).
Recent BH observations draw even larger attention to the study of BH f
ormation and evolution processes.
Unified picture of BH accretion flows and jets is still under construction.
Multi-wavelength variability properties and theory.
Observability of general relativistic effects.
New eyes to observe astrophysical black holes.
(Session 7)
(Sessions 5 & 8)
(Session 6)
(Sessions 5 & 8)
(Sessions 3 & 4) (All sessions)
(All sessions)
Organization and SupportOrganization and Support
Organized by • Kyoto University (Dept. of Physics, Yukawa Institute)• University of Tokyo (Dept. of Physics)• ISAS
Supported by • Grant-in-aid of Monbu-Kagakushou (MEXT) in Japan: “ Ne
w Development in Black Hole Astronomy” (K. Makishima)
• 21 Century COE Grant of Monbu-Kagakushou (MEXT): “ Center for Universality and Diversity of Physics” (K. Koyama)
• Yukawa Institute for Theoretical Physics
From the LOC…From the LOC…
Poster sessions • Poster rooms (Room 1/2) will be available from ~ 12:00am, t
oday until ~ 12:00am on the last day.• Coffee/tea service (in the afternoon break) in the poster room.
Support desk • Support desk is open until tomorrow, 5:00pm.
Other remarks • Please do not carry drinks to this event hall.• If you don’t mind, we wish to collect your presentation file after
your talk. It will be posted in the conference web-site.